All Figures

$\begin{figure} \par\includegraphics[width=11.7cm,clip]{9866f1.ps} \end{figure}$ Figure 1: The 6.3 $^\prime$ $\times$ 6.3 $^\prime$ field of view around WFI J2033-4723. This image is the central part of a combination of 418 R-band frames obtained with the 1.2 m EULER Telescope with a total exposure time of 48 h and a mean seeing of 1.3 $^{\prime \prime }$ . The three stars PSF1-3 used to model the Point Spread Function (PSF) and the 7 reference stars S4-10 used for frame alignment and flux calibration are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9866f2.ps}\end{figure}$ Figure 2: Result of the simultaneous deconvolution of the 956 R-band images (EULER+SMARTS) of WFI J2033-4723. The pixel size of this image is half the pixel size of the EULER detector, i.e., 0.172 $^{\prime \prime }$ , and the resolution is 2 pixels Full-Width-Half-Maximum, i.e., 0.344 $^{\prime \prime }$ . The field of view is 22 $^{\prime \prime }$ on a side. Two galaxies G2 and G3 are seen to the West and North of the main lensing galaxy G1. G3 is part of a group included in the lens modeling, while G1 and G2 are modeled individually (see Sect. 5).
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In the text

$\begin{figure} \par\includegraphics[width=12.2cm,clip]{9866f3.ps}\end{figure}$ Figure 3: Our R-band light curves obtained for WFI J2033-4723 as well as for the reference star S6 (see Fig. 1). The magnitudes are given in relative units. The filled symbols correspond to the EULER observations while the SMARTS data points are marked by open symbols. Components A₁ and A₂ were summed into one single component A. The curves have been shifted in magnitude for visibility, as indicated in the figure.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{9866f4a.ps}\includegraphic... ....7cm,clip]{9866f4b.ps}\includegraphics[width=5.7cm,clip]{9866f4c.ps}\end{figure}$ Figure 4: Left: deep NICMOS2 image, taken in the F160W-band. This image is a combination of 4 frames, for a total exposure time of 46 min. North is up and East to the left. The field of view is 4 $^{\prime \prime }$ on a side. Middle: simultaneous deconvolution of the individual NICMOS images (see text), using the MCS deconvolution algorithm. The PSF in this image is an analytical Gaussian with 2 pixels Full-Width-at-Half-Maximum ( FWHM), i.e., the resolution is 0.075 $^{\prime \prime }$ . The pixel size is 0.035 $^{\prime \prime }$ , i.e., oversampled by a factor of two compared to the original pixel size. Right: residual map of the deconvolution, with the cut levels set to $\pm$ $5\sigma$ . Only minor structures are seen in the center of the sharpest objects, which is acceptable given the quality of the NICMOS PSF.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9866f5.ps}\end{figure}$ Figure 5: Example of a dispersion curve as obtained from the minimum dispersion method, for components B and A. The position of the parabola minimum gives the time delay. Each point is separated by 2 days, i.e. about half the data mean sampling. The time delay indicated here is for only one realization of the boot-strap procedure (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9866f6a.ps}\vspace*{3mm} \includegraphics[width=7.6cm,clip]{9866f6b.ps}\end{figure}$ Figure 6: Variation of the dispersion function minimum $D_{{\rm min}}$ (red solid curves), as a function of the magnitude shift used for the normalization (see Sect. 4.1). Each $D_{{\rm min}}$ corresponds to a different estimate of the time delay, indicated on the blue dotted curves. The final time delay is the one with the lowest $D_{{\rm min}}$ . The top panel is for the B-A time delay, the bottom one for B-C. Time delays indicated here are for only one realization of the boot-strap procedure (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9866f7a.ps}\vspace*{3mm} \includegraphics[width=7.5cm,clip]{9866f7b.ps} \end{figure}$ Figure 7: Top: best polynomial fit to the light curves, which are shifted vertically for display purpose. Bottom: the residuals of the fit.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9866f8a.ps}\vspace*{3mm} \includegraphics[width=7.5cm,clip]{9866f8b.ps} \end{figure}$ Figure 8: Top: the light curves of the quasar images shown along with the best numerical model. Bottom: the residuals of the fit.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9866f9.ps}\end{figure}$ Figure 9: Light curves of the three quasar images, shifted by their respective time delay and flux ratio. The blue circles correspond to image A, the red triangles to B and the green squares to C.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9866f10.ps} \end{figure}$ Figure 10: Environment of WFI J2033-4723 as seen in an HST/ACS F814 (I-band) image. The main lens galaxy G1 and the close companion G2 were included in our analysis of the NICMOS image, and here we have labeled additional group members as G3-G6.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9866f11.ps} \end{figure}$ Figure 11: Distribution of $H_{\rm0}$ from 1000 non-parametric models. The bottom-axis gives the Hubble time, the top-axis $H_{\rm0}$ in km s^-1 Mpc^-1.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{9866f12.eps} \end{figure}$ Figure 12: Mean mass distribution from 1000 pixellated lens models. The red dots are the quasar images and the blue dot the source position. The thick solid line indicates the observed major axis of the lensing galaxy. Each tick-mark measures 1 $^{\prime \prime }$ . The third contour from the outside traces the critical mass density $\Sigma _{\rm crit} = 1.19$ $\times$ $10^{11}~M_{\odot}$ arcsec^-2, and the others are drawn logarithmically from the critical one (each contour is 2.5 larger/smaller than the previous one). North is to the top and East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9866f5.ps}\end{figure}$	Figure 5: Example of a dispersion curve as obtained from the minimum dispersion method, for components B and A. The position of the parabola minimum gives the time delay. Each point is separated by 2 days, i.e. about half the data mean sampling. The time delay indicated here is for only one realization of the boot-strap procedure (see text).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9866f7a.ps}\vspace*{3mm} \includegraphics[width=7.5cm,clip]{9866f7b.ps} \end{figure}$	Figure 7: Top: best polynomial fit to the light curves, which are shifted vertically for display purpose. Bottom: the residuals of the fit.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9866f8a.ps}\vspace*{3mm} \includegraphics[width=7.5cm,clip]{9866f8b.ps} \end{figure}$	Figure 8: Top: the light curves of the quasar images shown along with the best numerical model. Bottom: the residuals of the fit.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9866f9.ps}\end{figure}$	Figure 9: Light curves of the three quasar images, shifted by their respective time delay and flux ratio. The blue circles correspond to image A, the red triangles to B and the green squares to C.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9866f10.ps} \end{figure}$	Figure 10: Environment of WFI J2033-4723 as seen in an HST/ACS F814 (I-band) image. The main lens galaxy G1 and the close companion G2 were included in our analysis of the NICMOS image, and here we have labeled additional group members as G3-G6.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9866f11.ps} \end{figure}$	Figure 11: Distribution of $H_{\rm0}$ from 1000 non-parametric models. The bottom-axis gives the Hubble time, the top-axis $H_{\rm0}$ in km s^-1 Mpc^-1.
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